Transition region and coronal plasmas: instrumentation and spectral analysis

Details Transition region and coronal plasmas: instrumentation and spectral analysis Transition region and coronal plasmas: instrumentation and spectral analysis

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002ap%26ss.282..189w&link_type=abstract

Astrophysics and Space Science, v. 282, Issue 1, p. 189-207 (2002).

Astronomy and Astrophysics

Astrophysics

8

Solar Wind, Sun: Corona, Sun: Transition Region, Sun: Uv Radiation

Scientific paper

The plasma conditions in the solar atmosphere and, in particular, in coronal holes are summarized, before space-borne instrumentation for observing these regions in vacuum-ultraviolet light is briefly introduced with the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on the Solar and Heliospheric Observatory (SOHO) as example. Spectroscopic measurements of small plasma jets are then analyzed in detail. Magnetic reconnection is thought to be responsible for heating the corona of the Sun as well as accelerating the solar wind by converting magnetic energy into thermal and kinetic energies. The continuous outflow of the fast solar wind from coronal holes on ‘open’ field lines, which reach out into interplanetary space, then requires many reconnection events of very small scale sizes - most of them probably below the resolution capabilities of present-day instruments. Our observations of such an event have been obtained with the Solar and Heliospheric Observatory (SOHO) providing both high-resolution imaging and spectral information for structural and dynamical studies. We find whirling or rotating motions as well as jets with acceleration along their propagation paths in close spatial and temporal vicinity to the coronal jet.

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